Multiplicity is an integral and ubiquitous aspect of the star formation process [1]}. The broad diversity of multiple systems suggests that there most likely are several processes responsible for the formation of different types of binaries. Given the low likelihood of dynamical capture and the prevalence of dense cores hosting multiple protostars [2]}, it is generally assumed that visual binaries, with separations \(\gtrsim 10\)  au, result from the fragmentation of a prestellar core prior to, or during, its initial collapse [3]}. The properties of multiple systems and their dependency on stellar mass, age and environment encode the physics at play during star formation. From the theoretical perspective, understanding how the initial fragmentation and subsequent accretion on the stellar seeds relate to the final properties of the multiple system is an ongoing effort [4]}.
